3D turbulent reconnection: Theory, tests, and astrophysical implications

@article{Lazarian20203DTR,
  title={3D turbulent reconnection: Theory, tests, and astrophysical implications},
  author={Alex Lazarian and Gregory L. Eyink and Amir Jafari and Grzegorz Kowal and Hui Li and Siyao Xu and Ethan T. Vishniac},
  journal={Physics of Plasmas},
  year={2020}
}
Magnetic reconnection, topological changes in magnetic fields, is a fundamental process in magnetized plasmas. It is associated with energy release in regions of magnetic field annihilation, but this is only one facet of this process. Astrophysical fluid flows normally have very large Reynolds numbers and are expected to be turbulent, in agreement with observations. In strong turbulence, magnetic field lines constantly reconnect everywhere and on all scales, thus making magnetic reconnection an… 
Probing Magnetic Field Morphology in Galaxy Clusters with the Gradient Technique
Magnetic fields in the intracluster medium (ICM) affect the structure and the evolution of galaxy clusters. However, their properties are largely unknown, and measuring magnetic fields in galaxy
MHD Turbulence: A Biased Review
This review puts the developments of the last few years in the context of the canonical time line (Kolmogorov to Iroshnikov-Kraichnan to Goldreich-Sridhar to Boldyrev). It is argued that Beresnyak's
Solar Wind Turbulence Outlined Through Magnetic Islands and Nonlinear Waves
Various space missions and observations over the past decades have provided unexampled details about the nature of solar wind, the acceleration mechanism, and different nonlinear phenomena
Magnetic reconnection: MHD theory and modelling
In this review we focus on the fundamental theory of magnetohydrodynamic reconnection, together with applications to understanding a wide range of dynamic processes in the solar corona, such as
Chaos, complexity, and intermittent turbulence in space plasmas
Intermittent turbulence is key for understanding the stochastic nonlinear dynamics of space, astrophysical, and laboratory plasmas. We review the observation and theory of chaos and complexity in
Measurement of MHD Turbulence Properties by Synchrotron Radiation Techniques
It is well known that magnetohydrodynamic (MHD) turbulence is ubiquitous in astrophysical environments. The correct understanding of the fundamental properties of MHD turbulence is a pre-requisite
The Stationary Electric Field in the Heliosphere and Its Possible Relation to Current Sheets
The nature of the large-scale electric field in the heliosphere is discussed in this paper. The electric potential along each line of the magnetic field should be constant in the ideally conductive
Local analysis of fast magnetic reconnection
Fast magnetic reconnection is defined by the topology of the magnetic field lines changing on a timescale that is approximately an order of magnitude longer than the topology-conserving
Magnetic reconnection in the era of exascale computing and multiscale experiments
Astrophysical plasmas have the remarkable ability to preserve magnetic topology, which inevitably gives rise to the accumulation of magnetic energy within stressed regions including current sheets.
...
...

References

SHOWING 1-10 OF 324 REFERENCES
Intensity Gradients Technique: Synergy with Velocity Gradients and Polarization Studies
Magnetic fields are ubiquitous in the interstellar medium but are notoriously difficult to study through observation. Making use of the advances in our understanding of MHD turbulence and turbulent
Magnetic stochasticity and diffusion.
TLDR
A connection is established between magnetic stochasticity S_{p}(t) and magnetic diffusion in magnetohydrodynamic (MHD) turbulence and a homogeneous, incompressible MHD simulation is used to test this prediction.
Recent Developments in Collisionless Reconnection Theory: Applications to Laboratory and Astrophysical Plasmas
Recent developments in the theory and simulation of nonlinear collisionless reconnection hold the promise for providing solutions to some outstanding problems in laboratory and astrophysical plasma
Topology and stochasticity of turbulent magnetic fields.
TLDR
The results support the well-founded yet partly overlooked picture in which magnetic reconnection in turbulent fluids occurs on a wide range of scales as a result of nonlinearities at large scales (turbulence inertial range) and nonidealities at small scales (dissipative range).
Magnetic reconnection with null and X-points
Null and X-points of magnetic fields are places at which magnetic field lines with fundamentally different topologies approach each other arbitrary closely before separating by a distance set by the
Diffusion regions and 3D energy mode development in spontaneous reconnection
The understanding of magnetic reconnection in three-dimension (3D) is far shallower than its counterpart in two-dimension (2D) due to its potential complication, not to mention the evolving of the
Prevalence of magnetic reconnection at small field shear angles in the solar wind
A study of magnetic reconnection exhausts observed at high (3‐s) temporal resolution by the plasma and magnetic field experiments on Wind during March 2006 reveals, unexpectedly, that reconnection in
Heliospheric magnetic field strength and polarity from 1 to 81 AU during the ascending phase of solar cycle 23
[1] The Voyager 1 (V1) observations of the heliospheric magnetic field strength B agree with Parker's model of the global heliospheric magnetic field from 1 to 81.0 AU and from 1978 to 2001.34 when
Stochastic Reconnection for Large Magnetic Prandtl Numbers
We consider stochastic magnetic reconnection in high-β plasmas with large magnetic Prandtl numbers, Pr m > 1. For large Pr m , field line stochasticity is suppressed at very small scales, impeding
...
...